Implications of our results for the formation of metal-rich worlds. (a) Probability p_GI that a late orbital instability forms metal-rich worlds as large and massive as the observed high-density exoplanets. The probability is computed as described in Section 2.4 and the planets are listed along the x-axis in order of increasing size. (b) Occurrence rate of the modeled metal-rich giant-impact remnants, η_MR, binned as a function of planetary radius, R. η_MR is computed as the fraction of the metal-rich worlds in the post-instability planetary population; the vertical bars indicate one standard deviation uncertainties computed across all simulation scenarios described in Table F.1. While most of the observed high-density exoplanets are too large to be metal-rich giant-impact remnants, sub-Earth-sized metal-rich worlds formed during a late orbital instabilities should be instead relatively common in the local galaxy but are likely too small to be detected by current exoplanetary surveys.