  (Abridged) We present maps for various Galactic longitudes and latitudes at
1.4 GHz, which is the frequency where deep SKA surveys are proposed. The maps
are about 1.5 deg in size and have an angular resolution of about 1.6 arcsec.
We analyse the maps in terms of their probability density functions (PDFs) and
structure functions. Total intensity emission is more smooth in the plane than
at high latitudes due to the different contributions from the regular and
random magnetic field. The high latitude fields show more extended polarized
emission and RM structures than those in the plane, where patchy emission
structures on very small scales dominate. The RM PDFs in the plane are close to
Gaussians, but clearly deviate from that at high latitudes. The RM structure
functions show smaller amplitudes and steeper slopes towards high latitudes.
These results emerge from the fact that much more turbulent cells are passed
through by the line-of-sights in the plane. Although the simulated random
magnetic field components distribute in 3D, the magnetic field spectrum
extracted from the structure functions of RMs conforms to 2D in the plane and
approaches 3D at high latitudes. This is partly related to the outer scale of
the turbulent magnetic field, but mainly to the different lengths of the
line-of-sights.
