﹩{M}_{{G}_{\mathrm{RP}}}﹩ vs. G_BP − G_RP for stars within the boundary of Sco–Cen defined by de Zeeuw et al. (1999) that have π > 5 mas, π/σ ≥ 20, and RUWE < 1.6 in Gaia DR2. We have selected a sample of candidate young, low-mass stars based on colors of G_BP − G_RP = 1.4–3.4 mag (∼0.15–1 M_⊙) and positions above the single-star sequence for the Tuc-Hor association (45 Myr, Bell et al. 2015; solid line). We have marked a reddening vector for the extinction curve from Schlafly et al. (2016) and the spectral types that correspond to these colors for young stars (see Appendix C).