  It has long been argued that the radial distribution of globular clusters
(GCs) in the Fornax dwarf galaxy requires its dark matter halo to have a core
of size $\sim 1$ kpc. We revisit this argument by investigating analogues of
Fornax formed in E-MOSAICS, a cosmological hydrodynamical simulation that
self-consistently follows the formation and evolution of GCs in the EAGLE
galaxy formation model. In EAGLE, Fornax-mass haloes are cuspy and well
described by the Navarro-Frenk-White profile. We post-process the E-MOSAICS to
account for GC orbital decay by dynamical friction, which is not included in
the original model. Dynamical friction causes 33 per cent of GCs with masses
$M_{\rm GC}\geq4\times10^4 {~\rm M_\odot}$ to sink to the centre of their host
where they are tidally disrupted. Fornax has a total of five GCs, an
exceptionally large number compared to other galaxies of similar stellar mass.
In the simulations, we find that only 3 per cent of the Fornax analogues have
five or more GCs, while 30 per cent have only one and 35 per cent have none. We
find that GC systems in satellites are more centrally concentrated than in
field dwarfs, and that those formed in situ (45 per cent) are more concentrated
than those that were accreted. The survival probability of a GC increases
rapidly with the radial distance at which it formed ($r_{\rm init}$): it is 37
per cent for GCs with $r_{\rm init} \leq 1$ kpc and 92 per cent for GCs with
$r_{\rm init} \geq 1$ kpc. The present-day radial distribution of GCs in
E-MOSAICS turns out to be indistinguishable from that in Fornax, demonstrating
that, contrary to claims in the literature, the presence of five GCs in the
central kiloparsec of Fornax does not exclude a cuspy DM halo.
