  The first X-ray observation of the Seyfert 2 galaxy NGC5252 is reported. ASCA
collected $\sim 4000$ photons/detector enough to perform an accurate spectral
analysis of this source. The luminosity of NGC5252 is L$_{\rm X}$(0.7-10 keV)
$\simeq 2.6 \times 10^{43}$ erg s$^{-1}$, typical of a Seyfert 1 galaxy. A
simple description of the spectrum with a single power law is ruled out by the
SIS data which shows a strong soft excess at E $\lsimeq$ 1.2 keV. The spectrum
is best fitted by models assuming either partial covering of the central source
or scattering of the X-ray continuum. The best-fit partial covering model
results in a flat ($\Gamma \simeq 1.45 \pm 0.2$) power law continuum emitted by
a source almost completely covered (at $\sim$ 94-97\%) by neutral matter
($N_{\rm H} \simeq (4.3 \pm 0.6) \times 10^{22}$ cm$^{-2}$). The detected iron
line is remarkably weaker (EW $\sim 90 \pm 60$ eV) than normally found from
Seyfert 2 galaxies. In an effort to interpret the observed flat spectrum with
an intrinsically steep power law as predicted by unified models, we also
included in the models neutral reflection, ionized absorption (warm absorber),
and non-uniform cold absorption (dual-absorber). We find that the observed flat
continum {\bf and} weakness of the iron line poses a problem for neutral
reflection models, whatever the assumed geometry is. The use of an ionized
absorber (scattering + warm-absorber model) instead of a neutral absorber seems
not justified with the present data. The ``dual-absorber'' model, representing
nonuniform (density) absorption along the line of sight, may provide an
alternative explanation for the flatness of the spectrum, with no constraints
on the Fe K emission line. Another plausible interpretation of the present data
is that the X-ray spectrum of NGC5252 is truly intrinsically flat. Its strong
