Star clusters form from infrared dark clouds as embedded objects.
When massive star formation occurs within the embedded cluster, the feedback from these stars
impacts its surrounding gas.
The ensuing interplay between self-gravity and stellar feedback results either in continuing
star formation, or cleaning the cluster of its natal gas in which case star formation is quenched.
Depending on the gas expulsion time-scale and the star formation efficiency, gas expulsion can have a profound
impact on star cluster dynamics, possibly unbinding a significant fraction of stars from the cluster.
Using hydrodynamic simulations including feedback in the from of stellar winds and ionising radiation, and
self-gravity with a realistic sink particle integration,
we find that the approximation of the source of the feedback strongly influences the gaseous dynamics.
In one model, we represent all the massive stars by a single source located at the cluster centre.
In the other model, we resolve the cluster to individual stars and follow their dynamics.
While the stellar feedback drives a single shell out of the cluster in the former model,
it forms a complicated network of sheets and filaments in the latter model, which slows down
the process of gas expulsion.
For example, an embedded cluster of total mass $3 \times 10^3 M_{\odot}$ expels its natal gas
on a timescale $t_{\rm ge}$ of $0.2$ Myr in the former model, while $t_{\rm ge}$ reaches $0.9$ Myr in the latter model.
The value of $t_{\rm ge}$ of the latter model is closer to observations,
which provide an estimate of $t_{\rm ge}$ of the order of $1$ to $2$ Myr.
Another finding which is in agreement with observations is that $t_{\rm ge}$ slightly decreases
for more massive clusters.
In our models, star clusters with central escape speed larger than $\approx 10$ km/s, which corresponds
to the sound speed in an HII region, cannot overcome their self-gravity by their stellar feedback.
This indicates that these clusters are formed either with higher star formation efficiency (SFE) than
adopted in this work (we use $\mathrm{SFE} = 1/3$), or that the clusters can form with relatively
low SFEs, but their gas is expelled by another feedback mechanism (e.g, radiation pressure), which
is not included in the present work.