  We study the edge-on galaxy NGC 5775, utilizing a 58.2 ks {\sl Chandra}
ACIS-S observation together with complementary {\sl HST} ACS, {\sl Spitzer}
IRAC and other multi-wavelength data sets. This edge-on galaxy, with its
disk-wide active star formation, is particularly well-suited for studying the
disk/halo interaction on sub-galactic scales. We detect 27 discrete X-ray
sources within the $D_{25}$ region of the galaxy, including an ultra-luminous
source with a 0.3-7 keV luminosity of $\sim7\times10^{40}\rm ergs s^{-1}$. The
source-removed diffuse X-ray emission shows several prominent extraplanar
features, including a $\sim10\rm kpc$ diameter ``shell-like'' feature and a
``blob'' reaching a projected distance of $\sim25\rm kpc$ from the galactic
disk. The bulk of the X-ray emission in the halo has a scale height of
$\sim$1.5 kpc and can be characterized by a two-temperature optically thin
thermal plasma with temperatures of $\sim$ 0.2 and 0.6 keV and a total 0.3-2
keV luminosity of $\sim3.5\times10^{39}\rm ergs s^{-1}$. The high-resolution,
multi-wavelength data reveal the presence of several extraplanar features
around the disk, which appear to be associated with the in-disk star formation.
We suggest that hot gas produced with different levels of mass loading can have
different temperatures, which may explain the characteristic temperatures of
hot gas in the halo. We have obtained a sub-galactic scale X-ray-intensity-star
formation relation, which is consistent with the integrated version in other
star forming galaxies.
