  We present continued results from a wide-field, ~150 deg^2, optical
photometric and spectroscopic survey of the northern part of the ~5 Myr-old
Upper Scorpius OB Association. Photometry and spectral types were used to
derive effective temperatures and luminosities and place newly identified
association members onto a theoretical Hertzsprung-Russell diagram. From our
survey, we have discovered 145 new low mass members of the association, and
determined ~10% of these objects to be actively accreting material from a
surrounding circumstellar disk. Based on comparison of the spatial
distributions of low and high mass association members, we find no evidence for
spatial segregation by mass within the northern portion of the association.
Measured data are combined with pre-main sequence evolutionary models to derive
a mass and age for each star. Using Monte Carlo simulations we show that,
taking into account known observational uncertainties, the observed age
dispersion for the low mass population in USco is consistent with all stars
forming in a single burst ~5 Myr ago, and place an upper limit of +/-3 Myr on
the age spread if the star formation rate has been constant in time. We derive
the first spectroscopic mass function for USco that extends into the substellar
regime, and compare these results to those for three other young clusters and
associations.
