Dynamical architecture of stable and unstable planetary systems anchored at the disk inner edge at the end of the simulations (50 Myr). From left to right, the top panels: cumulative distributions of period ratio, mass, and orbital eccentricity. From left to right, the bottom panels: distributions of orbital inclination and number of planets. Only planets with semi-major axes smaller than 0.7 AU and masses larger than 1 M_⊕ are considered. In all considered models Rocky_peb = 0.1 cm. The Kepler planet mass distribution inferred from the mass–radius relationship of Wolfgang et al. (2016) is shown as a thick gray line. The uncertainty in the mass distribution is shown by the thin gray lines (M ± σ_M).