  We present the analysis of the magnetic field ($B$-field) structure of
galaxies measured with far-infrared (FIR) and radio (3 and 6 cm) polarimetric
observations. We use the first data release of the Survey on extragALactic
magnetiSm with SOFIA (SALSA) of 14 nearby ($<20$ Mpc) galaxies with resolved (5
arcsec-18 arcsec; $90$ pc--$1$ kpc) imaging polarimetric observations using
HAWC+/SOFIA from $53$ to $214$ \um. We compute the magnetic pitch angle
($\Psi_{B}$) profiles as a function of the galactrocentric radius. We introduce
a new magnetic alignment parameter ($\zeta$) to estimate the
disordered-to-ordered $B$-field ratio in spiral $B$-fields. We find FIR and
radio wavelengths to not generally trace the same $B$-field morphology in
galaxies. The $\Psi_{B}$ profiles tend to be more ordered with galactocentric
radius in radio ($\zeta_{\rm{6cm}} = 0.93\pm0.03$) than in FIR
($\zeta_{\rm{154\mu m}} = 0.84\pm0.14$). For spiral galaxies, FIR $B$-fields
are $2-75$\% more turbulent than the radio $B$-fields. For starburst galaxies,
we find that FIR polarization is a better tracer of the $B$-fields along the
galactic outflows than radio polarization. Our results suggest that the
$B$-fields associated with dense, dusty, turbulent star-forming regions, those
traced at FIR, are less ordered than warmer, less-dense regions, those traced
at radio, of the interstellar medium. The FIR $B$-fields seem to be more
sensitive to the activity of the star-forming regions and the morphology of the
molecular clouds within a vertical height of few hundred pc in the disk of
spiral galaxies than the radio $B$-fields.
