Gas accretion rate as a function of dust disc mass for protoplanetary discs formed from cloud cores with masses and final centrifugal radii shown in Table 1. The yellow and blue lines trace the time evolution of the cases with the lowest and highest mass, and lowest and highest centrifugal radius, respectively. As a general trend, discs from low-mass cloud cores evolve faster than those from higher-mass cloud cores. However, the speed with which the disc evolves also depends on the final centrifugal radius. At 3 Myr (panel d), all dust discs except for the ones coming from 2 M_⊙ cloud cores have been completely drained out.