Sketch of the global framework explored in this work. Disc evolution through angular momentum extraction by an MHD wind with additional low-level internal and external photoevaporation with accretion occurring in layers at the disc surface. Low-mass planets remain embedded and undergo type I migration. Growing planets eventually open a gap and transition to type II migration. Initially, the fast accretion layer bypasses the planet, which migrates due to Lindblad torques from the gap (viscosity-dominated regime), while still accreting. At higher masses, the planet fully blocks the flow, entering wind-driven type II migration, where it is pushed by the outer gap replenished by the accretion flow.