Dynamical evolution of protoplanetary embryos in a simulation of Model I where t_start = 0.5 Myr, S_peb = 1 and the size of the rocky pebbles is Rocky_peb = 0.1 cm (same simulation as in Fig. 3). Top left-hand panel: evolution of the semi-major axes. Top right-hand panel: evolution of the eccentricities. Bottom left-hand and right-hand panels: mass growth and the orbital inclinations, respectively. The dashed vertical line shows the end of the gas disk dispersal (corresponding to Ṁ ~ 10⁻⁹M_⊙ yr⁻¹ in Eq. (2)). Colored lines show the final planets inside 0.7 AU. The gray line shows final planets and leftover protoplanetary embryos with orbits outside 0.7 AU. Leftover embryos are those with masses smaller than ~ 0.1 M_⊕. Finally, the black line shows collided or ejected objects over the course of the simulation.