Variation in the 2 M_⊙ star CESAM2K20 models presented in Fig. 2 based on a variety of criteria, including: (i) metallicity, (ii) above core convective overshooting, (iii) mean surface rotation velocity during the MS, and (iv) radiative acceleration (see Sect. 4.3 for more details). For the metallicity case, we have elected to also include the 1.9 M_⊙ star CESAM2K20 model as a comparison.