  We present the first high signal-to-noise broadband X-ray spectrum of the
radio-quiet type-2 Seyfert ESO 033-G002, combining data from $XMM$-$Newton$ and
$NuSTAR$. The nuclear X-ray spectrum is complex, showing evidence for both
neutral and ionised absorption, as well as reflection from both the accretion
disc and more distant material, but our broadband coverage allows us to
disentangle all of these different components. The total neutral column during
this epoch is $N_{\rm{H}} \sim 5-6 \times 10^{22}$ cm$^{-2}$, consistent with
the optical classification of ESO 033-G002 as a type-2 Seyfert but not so large
as to prevent us from robustly determining the properties of the innermost
accretion flow. The ionised absorption - dominated by lines from Fe XXV and Fe
XXVI - reveals a moderately rapid outflow ($v_{\rm{out}} \sim 5400$ km
s$^{-1}$) which has a column comparable to the neutral absorption. We find the
disc reflection from the innermost regions to be extreme, with a reflection
fraction of $R_{\rm{frac}} \sim 5$. This requires strong gravitational
lightbending and, in turn, both an extremely compact corona (within $\sim$2
$R_{\rm{G}}$ of the black hole) and a rapidly rotating black hole ($a^* >
0.96$). Despite this tight size constraint, with a temperature of $kT_{\rm{e}}
= 40-70$ keV the X-ray corona in ESO 033-G002 appears similar to other AGN in
terms of its placement in the compactness-temperature plane, consistent with
sitting close to the limit determined by runaway pair production. Finally,
combining X-ray spectroscopy, timing and updated optical spectroscopy, we also
estimate the mass of the black hole to be $\log[M_{\rm{BH}} / M_{\odot}] \sim
7.0 - 7.5$.
