Schematic of the model setup of this work. We modelled the evolution of feedback-driven bubbles, formed by the winds and supernovae from the star cluster forming at the centre. The scheme presents a cone of the otherwise spherically symmetric bubble structure, showing the location of the reverse (R_rs) and forward shocks (R_sh), and the contact discontinuity (R_cd) that separates shocked wind from ambient swept-up gas. Furthermore, the dashed arrows indicate the directions of the different forces that determine the evolution of the shell radius: the inward gravitational force (F_g) and ram pressure from the cloud (F_cl), and the outward force produced by the thermal energy of the hot bubble (F_th). This term was calculated by considering radiative cooling within the bubble (Q_w), which includes the effect of mass evaporation from the cold shell. The evaporated material (${\dot{M}}_{\text{ev}}$) mass-loads the bubble interior, thus modifying its density and temperature structure and, consequently, the cooling rate. In addition, our model setup includes star formation in the shell (not included for clarity of the diagram). See the text for details.