Mass segregation ratios Λ and masses of N_MST most massive stars for an older subset of the stellar populations. Same as Figure 1, but only considering stars formed before 0.75 t_collapse, indicated by the red dotted line. The three rows correspond to the M4, M5, and M6 models as labeled. In each row: (top) mass segregation ratio Λ over time for the N_MST most massive stars in each cluster. The vertical dotted white lines indicate the time of collapse, where R_rms reaches a minimum. The solid white lines correspond to the right vertical axis showing the stellar mass of the cluster. (bottom) mass of the N_MST^th most massive star in each cluster. The grey vertical lines indicate the formation of a new most-massive star (N_MST = 1). As these are often not in the core, the time of formation, particularly in M4, corresponds to a drop in the apparent mass segregation. Note that each cluster was run to ≈ 1.5t_ff, leading to different absolute timescales.