  We present optical integral field spectroscopy of the circum-nuclear gas of
the Seyfert 2 galaxy NGC 1386. The data cover the central 7$^{\prime\prime}
\times 9^{\prime\prime}$ (530 $\times$ 680 pc) at a spatial resolution of 0.9"
(68 pc), and the spectral range 5700-7000 \AA\ at a resolution of 66 km
s$^{-1}$. The line emission is dominated by a bright central component, with
two lobes extending $\approx$ 3$^{\prime\prime}$ north and south of the
nucleus. We identify three main kinematic components. The first has low
velocity dispersion ($\bar \sigma \approx $ 90 km s$^{-1}$), extends over the
whole field-of-view, and has a velocity field consistent with gas rotating in
the galaxy disk. We interpret the lobes as resulting from photoionization of
disk gas in regions where the AGN radiation cones intercept the disk. The
second has higher velocity dispersion ($\bar \sigma \approx$ 200 km s$^{-1}$)
and is observed in the inner 150 pc around the continuum peak. This component
is double peaked, with redshifted and blueshifted components separated by
$\approx$ 500 km s$^{-1}$. Together with previous HST imaging, these features
suggest the presence of a bipolar outflow for which we estimate a mass outflow
rate of $\mathrm{\dot M} \gtrsim $ 0.1 M$_{\odot}$ yr$^{-1}$. The third
component is revealed by velocity residuals associated with enhanced velocity
dispersion and suggests that outflow and/or rotation is occurring approximately
in the equatorial plane of the torus. A second system of velocity residuals may
indicate the presence of streaming motions along dusty spirals in the disk.
