We present results of a spectroscopic survey for new K- and M-type members of Scorpius-Centaurus ( Sco-Cen ) , the nearest OB Association ( \sim 100–200 pc ) . Using an X-ray , proper motion and color-magnitude selected sample , we obtained spectra for 361 stars , for which we report spectral classifications and Li and H \alpha equivalent widths . We identified 156 new members of Sco-Cen , and recovered 51 previously published members . We have combined these with previously known members to form a sample of 493 solar-mass ( \sim 0.7–1.3 M _ { \odot } ) members of Sco-Cen . We investigated the star-formation history of this sample , and re-assessed the ages of the massive main-sequence turn-off and the G-type members in all three subgroups . We performed a census for circumstellar disks in our sample using WISE infrared data and find a protoplanetary disk fraction for K-type stars of 4.4 ^ { +1.6 } _ { -0.9 } % for Upper Centaurus-Lupus and Lower Centaurus-Crux at \sim 16 Myr and 9.0 ^ { +4.0 } _ { -2.2 } % for Upper Scorpius at \sim 10 Myr . These data are consistent with a protoplanetary disk e-folding timescale of \sim 4–5 Myr for \sim 1 M _ { \odot } stars , twice that previously quoted ( Mamajek 2009 ) , but consistent with the Bell et al . revised age scale of young clusters . Finally , we construct an age map of Scorpius-Centaurus which clearly reveals substructure consisting of concentrations of younger and older stars . We find evidence for strong age gradients within all three subgroups . None of the subgroups are consistent with being simple , coeval populations which formed in single bursts , but likely represents a multitude of smaller star formation episodes of hundreds to tens of stars each .