Upper panels: time evolution of the gas surface density profiles for massive (top), intermediate (middle), and low (bottom) mass discs around stars with masses between 1 M_⊙ and 3 M_⊙ in discs with α₀ = 10⁻², plotted every 0.1 Myr. The labels at the top right of each panel represent the simulation number and the dissipation timescale, also represented by the colour scale bar shown on the vertical right-hand side of the plot. The coloured simulation numbers refer to specific cases described in the text. Lower panels: time evolution of the mass accretion rate Ṁ_acc (solid red curve) and the mass-loss rates Ṁ_X (solid blue curve) and Ṁ_FUV (solid lilac curve) by the X-ray and FUV photoevaporation, respectively, for the same discs, integrated along the regions where there is still gas surface density to remove. The dashed blue and lilac curves represent the same mass-loss rates but integrated along the disc domain. The vertical dashed lines represent the time at which the gap opened in the disc, due to the effects of either X-ray (blue) or FUV (lilac) photoevaporation. For the high viscosity parameter assumed here, most discs evolve following the classical inside-out disc dispersal (see Sect. 3.1). Only for the highest stellar and disc masses (see cases S38 and S39) do the outer and inner discs disappear on similar timescales (a pathway that we call homogeneous disc evolution).