Same as Figure 2 but with the addition of a spread in the initial correlations between the disc properties and the stellar mass $({\sigma }_{M_{\mathrm{d}}}(0)=0.65$ dex, ${\sigma }_{R_{\mathrm{d}}}(0)=0.52$ dex). Despite the linear correlation being readily broken in theory (see Section 3.3), the scatter introduced by the spread in the initial conditions simulates the correlation also at more evolved ages. As an example, we show the fitted line at 5 Myr (the age of the oldest observed population) in both panels (log₁₀(M_d/M_⊙) = 3.1 log₁₀(M_*/M_⊙) − 3.3, ${\log }_{10}\left(\dot{M}/M_{\odot }{\mathrm{y}\mathrm{r}}^{-1}\right)=2.5$ log₁₀(M_*/M_⊙) − 10.4).