  Angular power spectra are calculated and presented for the entirety of the
Canadian Galactic Plane Survey polarization dataset at 1.4 GHz covering an area
of 1060 deg$^2$. The data analyzed are a combination of data from the 100-m
Effelsberg Telescope, the 26-m Telescope at the Dominion Radio Astrophysical
Observatory, and the Synthesis Telescope at the Dominion Radio Astrophysical
Observatory, allowing all scales to be sampled down to arcminute resolution.
The resulting power spectra cover multipoles from $\ell \approx 60$ to $\ell
\approx 10^4$ and display both a power-law component at low multipoles and a
flattening at high multipoles from point sources. We fit the power spectrum
with a model that accounts for these components and instrumental effects. The
resulting power-law indices are found to have a mode of 2.3, similar to
previous results. However, there are significant regional variations in the
index, defying attempts to characterize the emission with a single value. The
power-law index is found to increase away from the Galactic plane. A transition
from small-scale to large-scale structure is evident at $b= 9^{\circ}$,
associated with the disk-halo transition in a 15$^{\circ}$ region around
$l=108^{\circ}$. Localized variations in the index are found toward HII regions
and supernova remnants, but the interpretation of these variations is
inconclusive. The power in the polarized emission is anticorrelated with bright
thermal emission (traced by H$\alpha$ emission) indicating that the thermal
emission depolarizes background synchrotron emission.
