  We present full volume cosmological simulations using the moving-mesh code
AREPO to study the coevolution of dust and galaxies. We extend the dust model
in AREPO to include thermal sputtering of grains and investigate the evolution
of the dust mass function, the cosmic distribution of dust beyond the
interstellar medium, and the dependence of dust-to-stellar mass ratio on
galactic properties. The simulated dust mass function is well-described by a
Schechter fit and lies closest to observations at $z = 0$. The radial scaling
of projected dust surface density out to distances of $10 \, \text{Mpc}$ around
galaxies with magnitudes $17 < i < 21$ is similar to that seen in Sloan Digital
Sky Survey data, albeit with a lower normalisation. At $z = 0$, the predicted
dust density of $\Omega_\text{dust} \approx 1.3 \times 10^{-6}$ lies in the
range of $\Omega_\text{dust}$ values seen in low-redshift observations. We find
that dust-to-stellar mass ratio anti-correlates with stellar mass for galaxies
living along the star formation main sequence. Moreover, we estimate the $850
\, \mu\text{m}$ number density functions for simulated galaxies and analyse the
relation between dust-to-stellar flux and mass ratios at $z = 0$. At high
redshift, our model fails to produce enough dust-rich galaxies, and this
tension is not alleviated by adopting a top-heavy initial mass function. We do
not capture a decline in $\Omega_\text{dust}$ from $z = 2$ to $z = 0$, which
suggests that dust production mechanisms more strongly dependent on star
formation may help to produce the observed number of dusty galaxies near the
peak of cosmic star formation.
