Simulation results for the disc gap at 75 au and δ = 10⁻⁵, which ended from t₀ + 2.4 × 10⁵ to t₀ + 3.1 × 10⁵ yr. (a) e-m time sequence, showing that a small number of massive embryos started growth early and stirred the majority of the late-forming planetesimals into eccentric orbits, (b) i-m plot at the end of the simulations, showing that the i of all bodies remains far lower than the pebble disc scale height and confirms that the pebble relative velocity is critical, (c) Compared to the case of r₀ = 10 au and δ = 10⁻⁵, the differential mass distribution shows an even smaller number of massive cores formed in these simulations.