  The mass accretion rate is a crucial parameter for the study of the evolution
of accretion discs around young low-mass stellar and substellar objects (YSOs).
We revisit the case of MYLup, an object where VLT/X-Shooter data suggested a
negligible mass accretion rate, and show it to be accreting on a level similar
to other ClassII YSOs in Lupus based on HST observations. In our HST-COS and
-STIS spectra, we find many emission lines, as well as substantial FUV
continuum excess emission, which can be ascribed to active accretion. The total
luminosity of the CIV 1549A doublet is 4.1$\times10^{-4}$ Lsun. Using scalings
between accretion luminosity, Lacc, and CIV luminosity from the literature, we
derive Lacc $\sim$2$\times10^{-1}$ Lsun, which is more than an order of
magnitude higher than the upper limit estimated from the X-Shooter
observations. We discuss possible reasons for the X-Shooter-HST discrepancy,
the most plausible being that the low contrast between the continuum excess
emission and the photospheric+chromospheric emission at optical wavelengths in
MYLup hampered detection of excess emission. The luminosity of the FUV
continuum and CIV lines, strong H$_{2}$ fluorescence, and a "1600 A Bump" place
MYLup in the class of accreting objects with gas-rich discs. So far, MYLup is
the only peculiar case in which a significant difference between the HST and
X-Shooter Macc estimates exists that is not ascribable to variability. The mass
accretion rate inferred from the revisited Lacc estimate is Macc $\sim$ 1(
$^{+1.5}_{-0.5}$ )$\times10^{-8}$ Msun/yr. This value is consistent with the
typical value derived for accreting YSOs of similar mass in Lupus and points to
less clearing of the inner disc than indicated by near- and mid-infrared
observations. This is confirmed by ALMA data, which show that the gaps and
rings seen in the sub-millimetre are relatively shallow.
