Stellar accretion rate Ṁ_acc vs. gas disc mass M_disc shown for all disc wind scenarios (see Table 1) with a weak FUV field strength distribution. Evolution tracks of individual systems, coloured by ℱ_FUV, and snapshots at 2 Myr (green circles and 3 Myr (orange circles are displayed. Tracks of exemplary cases are highlighted with black dashed and dotted lines. We show the detailed evolution of those exemplary discs in Figs. 3 and 4. 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 M_disc/Ṁ_acc are shown for 0.1, 1 and 10 Myr (thin dotted lines).