Relation between the time t elapsed since the onset of star formation in the simulations and the mean age of the stellar component. Owing to the ongoing gas depletion and the star formation slow down that it induces, the mean age is slightly older than half the simulation time span. The bottom x-axis shows the physical time (i.e. time in units of Myr) while the top x-axis shows time in units of the initial local free-fall time at the clump half-mass radius, τ_ff(t = 0,r_hm) when p₀ = 1.7.