  Dynamically, cosmic rays with energies above about one GeV/nucleon may be
important agents of galaxy evolution. Their pressures compare with the thermal
and magnetic ones impacting galactic gas accretion, fountains and galactic
outflows, and alter the mass cycling between the gas phases, its efficiency
depends on the properties of CR transport in the different media. We aim to
study the dynamical role of CRs in shaping the interstellar medium of a galaxy
when changing their propagation mode. We perform MHD simulations with the AMR
code RAMSES of the evolution of the same isolated galaxy (dwarf galaxy of
$10^{11}$ M$_{\odot}$ down to 9-pc resolution) and compare the impact of the
simplest cosmic-ray transport assumption of uniform diffusion. We have also
updated the observational relation seen between the $\gamma$-ray luminosities
and SFR of galaxies using the latest detection of Fermi LAT sources. We find
that the radial and vertical distributions, and mass fractions of the gas in
the different phases are marginally altered when changing CR transport. We
observe positive feedback of CR on the amplification of the magnetic field in
the inner half of the galaxy, except for fast isotropic diffusion. The increase
in CR pressure for slow or anisotropic diffusion can suppress star formation by
up to 50\%, but the dual effect of cosmic-ray pressure and magnetic
amplification can reduce star formation by a factor 2.5. The $\gamma$-ray
luminosities and SFR of the simulated galaxies are fully consistent with the
trend seen in the observations in the case of anisotropic $10^{27.5-29}$ cm$^2$
s$^{-1}$ diffusion and for isotropic diffusion slower or equal to $3 \times
10^{28}$cm$^2$ s$^{-1}$. These results, therefore, do not confirm claims of
very fast $10^{29-31}$ cm$^2$ s$^{-1}$ diffusion to match the Fermi LAT
observations.
