Finalplanetary mass as a function of the final planetary orbit for protoplanets starting to accrete at t = 0 in the massive planetesimal population model with two different planetesimal radii (50 and 5 km) and three values of the turbulent stirring coefficient (10⁻⁴, 10⁻⁵, and 10⁻⁶). The solid blue line (γ = 10⁻⁴/R_pla = 50 km) corresponds to a cut at t₀ = 0 of the upper right panel of Fig. 2. The planetesimal inclinations are here set as the maximum of the inclinations given by turbulent stirring and by mutual planetesimal scattering. Planetesimals with a nominal radius of 50 km can only form Jupiter-mass planets interior of 3 AU, even when the turbulent stirring is very weak with γ = 10⁻⁵ or extremelyweak with γ = 10⁻⁶, because of inclination stirring by mutual planetesimal scattering. Lowering the planetesimal radius to 5 km allows the formation of Jupiter analogues when the turbulent stirring coefficient is γ = 10⁻⁵ or γ = 10⁻⁶.