Stellar accretion rate vs. gas disc mass M_disc, analogous to Fig. 5, but without EUV radiation shielding. Exemplary cases are the same as in Figs. 3 and 4, but without EUV radiation shielding. Snapshots at 2 Myr (green circles) and 3 Myr (orange circles) are displayed. We compare our simulations with observed populations in Lupus and Chamaeleon I. Observational dust disc masses and stellar accretion rates are taken from Manara et al. (2019) and dust masses are converted to gas masses by assuming the standard dust-to-gas ratio of 0.01. Triangles denote upper limits on disc mass. Lines of constant are shown for 0.1, 1 and 10 Myr (thin dotted lines).