Time evolution of the disc fraction for different evolution scenarios, FUV field strengths $F_{\text{FUV},10{\text{G}}_0}$ and ${ℱ}_{\text{FUV,CygnOB2}}$, varying τ_acc and f_PAH. Note that in the strongly irradiated cases, a duration of star formation of 2 Myr is accounted for while the low irradiated cases stars are set at t = 0. Panels a and b show results from simulations with $F_{\text{FUV},10{\text{G}}_0}$ for τ_acc,0,short and τ_acc,0,long, alongside with a selected sample of observed disc fractions for low mass star forming regions. Panels c and d show the results of the strongly irradiated cases with ${ℱ}_{\text{FUV,CygnOB2}}$ for τ_acc,0,short and τ_acc,0,long, alongside with observed disc fraction in Cygnus OB2 and two additional high mass star forming regions. See Appendix A for a Table A.1 and discussion of the observational constraints.