  We investigate whether the galaxy and star formation model used for the
Auriga simulations can produce a realistic globular cluster (GC) population. We
compare statistics of GC candidate star particles in the Auriga haloes with
catalogues of the Milky Way (MW) and Andromeda (M31) GC populations. We find
that the Auriga simulations do produce sufficient stellar mass for GC
candidates at radii and metallicities that are typical for the MW GC system
(GCS). We also find varying mass-ratios of the simulated GC candidates relative
to the observed mass in the MW and M31 GC systems for different bins of
galactocentric radius-metallicity (r$_{\text{gal}}$ -[Fe/H]). Overall, the
Auriga simulations produce GC candidates with higher metallicities than the MW
and M31 GCS and they are found at larger radii than observed. The Auriga
simulations would require bound cluster formation efficiencies higher than ten
percent for the metal-poor GC candidates, and those within the Solar radius
should experience negligible destruction rates to be consistent with
observations. GC candidates in the outer halo, on the other hand, should either
have low formation efficiencies, or experience high mass loss for the Auriga
simulations to produce a GCS that is consistent with that of the MW or M31.
Finally, the scatter in the metallicity as well as in the radial distribution
between different Auriga runs is considerably smaller than the differences
between that of the MW and M31 GCSs. The Auriga model is unlikely to give rise
to a GCS that can be consistent with both galaxies.
