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The SILCC project (SImulating the Life-Cycle of molecular Clouds) aims at amore self-consistent understanding of the interstellar medium (ISM) on smallscales and its link to galaxy evolution. We simulate the evolution of themulti-phase ISM in a 500 pc x 500 pc x 10 kpc region of a galactic disc, with agas surface density of $\Sigma_{_{\rm GAS}} = 10 \;{\rm M}_\odot/{\rm pc}^2$.The Flash 4.1 simulations include an external potential, self-gravity, magneticfields, heating and radiative cooling, time-dependent chemistry of H$_2$ and COconsidering (self-) shielding, and supernova (SN) feedback. We explore SNexplosions at different (fixed) rates in high-density regions (peak), in randomlocations (random), in a combination of both (mixed), or clustered in space andtime (clustered). Only random or clustered models with self-gravity (whichevolve similarly) are in agreement with observations. Molecular hydrogen formsin dense filaments and clumps and contributes 20% - 40% to the total mass,whereas most of the mass (55% - 75%) is in atomic hydrogen. The ionised gascontributes <10%. For high SN rates (0.5 dex above Kennicutt-Schmidt) as wellas for peak and mixed driving the formation of H$_2$ is strongly suppressed.Also without self-gravity the H$_2$ fraction is significantly lower ($\sim$5%). Most of the volume is filled with hot gas ($\sim$90% within $\pm$2 kpc).Only for random or clustered driving, a vertically expanding warm component ofatomic hydrogen indicates a fountain flow. Magnetic fields have little impacton the final disc structure. However, they affect dense gas ($n\gtrsim 10\;{\rmcm}^{-3}$) and delay H$_2$ formation. We highlight that individual chemicalspecies, in particular atomic hydrogen, populate different ISM phases andcannot be accurately accounted for by simple temperature-/density-based phasecut-offs.

The SILCC (SImulating the LifeCycle of molecular Clouds) project: I. Chemical evolution of the supernova-driven ISM