  We present magnetohydrodynamic (MHD) simulations of the star-forming
multiphase interstellar medium (ISM) in stratified galactic patches with gas
surface densities $\Sigma_\mathrm{gas} =$ 10, 30, 50, and 100
$\mathrm{M_\odot\,pc^{-2}}$. The SILCC project simulation framework accounts
for non-equilibrium thermal and chemical processes in the warm and cold ISM.
The sink-based star formation and feedback model includes stellar winds,
hydrogen-ionising UV radiation, core-collapse supernovae, and cosmic ray (CR)
injection and diffusion. The simulations follow the observed relation between
$\Sigma_\mathrm{gas}$ and the star formation rate surface density
$\Sigma_\mathrm{SFR}$. CRs qualitatively change the outflow phase structure.
Without CRs, the outflows transition from a two-phase (warm and hot at 1 kpc)
to a single-phase (hot at 2 kpc) structure. With CRs, the outflow always has
three phases (cold, warm, and hot), dominated in mass by the warm phase. The
impact of CRs on mass loading decreases for higher $\Sigma_\mathrm{gas}$ and
the mass loading factors of the CR-supported outflows are of order unity
independent of $\Sigma_\mathrm{SFR}$. Similar to observations, vertical
velocity dispersions of the warm ionised medium (WIM) and the cold neutral
medium (CNM) correlate with the star formation rate as $\sigma_\mathrm{z}
\propto \Sigma_\mathrm{SFR}^a$, with $a \sim 0.20$. In the absence of stellar
feedback, we find no correlation. The velocity dispersion of the WIM is a
factor $\sim 2.2$ higher than that of the CNM, in agreement with local
observations. For $\Sigma_\mathrm{SFR} \gtrsim 1.5 \times
10^{-2}\,\mathrm{M}_\odot\,\mathrm{yr}^{-1}\,\mathrm{kpc}^{-2}$ the WIM motions
become supersonic.
