  (Abridged) We present the results from {\it ASCA} observations of NGC 3227
along with those from a {\it ROSAT} observation. The 0.6--10 keV continuum is
consistent with a powerlaw with $\Gamma \sim 1.6$, flatter than that typically
observed in Seyfert galaxies. Fe $K$-shell emission is observed with an EW and
profile typical of Seyfert 1 galaxies. The {\it ASCA} observations in 1993
reveal absorption by a screen $N_{H,z}^{ion} \simeq 3\times10^{21} cm^{-2}}$ of
ionized material with $U_X \simeq 0.01$. Joint analysis of the {\it ASCA} and
{\it ROSAT} data show an additional screen of neutral material instrinsic to
NGC 3227 with $N_{H,z}^{neu} \sim $few$\times10^{20} cm^{-2}}$. NGC 3227
exhibits spectral variability both within and between the observations, due to
short-term variability in the continuum emission and longer-term variability in
the absorption. Time-resolved spectroscopy show the continuum steepened by
$\Delta \Gamma \simeq 0.1$ during a flare of duration $\sim 10^4$s. The column
increased by a factor of $\sim10$ by the 1995 epoch, while the continuum is
consistent with that observed in 1993. The 1995 data also show evidence that
the warm absorber allows $\sim$10% of the nuclear emission to escape without
attenuation.
