Dynamical mechanisms responsible for stellar escapes as a function of the cluster mass. For each cluster mass, we plot two bar plots; the left bar plot represents ProCeps, the right bar plot represents lower mass stars. The colours indicate the relative number of stars in each group which escaped due to gas expulsion (blue), dynamical evaporation (green), dynamical ejection (red), and the rest which either terminated their core Helium burning within the cluster (for ProCeps) or are still present in the cluster by the age of 145 Myr (yellow). We note that in the least massive clusters (M_ecl ≲ 200 M_⊙), which mass segregate before t_d, lower mass stars and ProCeps react differently to gas expulsion: as M_ecl decreases, more low-mass stars are unbound, while fewer ProCeps are unbound. The figure is for clusters with R_g = 8 kpc and Z = 0.014.