  Magnetohydrodynamic (MHD) and photoevaporative winds are thought to play an
important role in the evolution and dispersal of planet-forming disks. Here, we
analyze high-resolution ($\Delta v \sim$ 7 kms$^{-1}$) optical spectra from a
sample of 115 T Tauri stars in the $\sim 5-10$ Myr Upper Sco association and
focus on the [O I]$\lambda$6300 and H$\alpha$ lines to trace disk winds and
accretion, respectively. Our sample covers a large range in spectral type and
we divide it into Warm (G0-M3) and Cool (later than M3) to facilitate
comparison with younger regions. We detect the [O I]$\lambda$6300 line in 45
out of 87 upper sco sources with protoplanetary disks and 32 out of 45 are
accreting based on H$\alpha$ profiles and equivalent widths. All [O I]
$\lambda$6300 Upper Sco profiles have a low-velocity (centroid $< -30$
kms$^{-1}$, LVC) emission and most (36/45) can be fit by a single Gaussian
(SC). The SC distribution of centroid velocities and FWHMs is consistent with
MHD disk winds. We also find that the Upper Sco sample follows the same
accretion luminosity$-$LVC [O I]$\lambda$6300 luminosity relation and the same
anti-correlation between SC FWHM and WISE W3-W4 spectral index as the younger
samples. These results indicate that accretion and disk winds coevolve and
that, as inner disks clear out, wind emission arises further away from the
star. Finally, our large spectral range coverage reveals that Cool stars have
larger FWHMs normalized by stellar mass than Warm stars indicating that [O
I]$\lambda$6300 emission arises closer in towards lower mass/lower luminosity
stars.
