Evolution of hot accreting models with Z = 0.0001, final masses of M_fin = 0.7 and 0.8 M_⊙, and ṁ = 10⁻⁵ M_⊙ yr⁻¹. Standard non-accreting models (grey lines) and reference cold LLC accreting models (M_seed = 10 M_J, R_seed = 3 R_⊙, ṁ = 10⁻⁵ M_⊙ yr⁻¹, black line) are also shown for comparison purposes. Top left panel: HR diagram. The position of models at 1 Myr (filled triangles) and 10 Myr (filled squares), deuterium burning region (thick magenta line), and the end of the accretion phase (cross) are marked. Top right panel: relative contribution to the total luminosity of the nuclear burning (L_nuc.), gravitational contraction, and expansion (L_gra.) as well as accretion (L_acc.) as a function of the stellar mass during the protostellar accretion phase. Bottom left panel: evolution of the surface radius (in solar units) and central temperature (in units of 10⁶ K) as a function of the stellar mass. Bottom right panel: relative mass coordinate at the bottom of the convective envelope as a function of the stellar mass.