Details of the evolution of the star cluster half-mass radius r_h for selected models. The results for lower mass clusters (M_cl(0) = 1400 M_⊙) are shown in the left panel, for more massive clusters (M_cl(0) = 4400 M_⊙) in the right panel. An estimated half-mass radius for a system assuming conservation of adiabatic invariants, i.e. r_h(0) ≈ r_h(0)(M_cl(0)+M_gas(0))/(M_cl(0)+M_gas(t)) ≈ 3r_h(0)/(1 + 2exp(−(t − t_d)/τ_M)), where the second equality follows from Eq. (27) in Paper I and SFE = 1/3, with the gas expulsion timescale τ_M = 1 Myr, is indicated by the yellow dotted line.