  We develop a model describing the dynamical and observed properties of
disc-dominated TDEs around black holes with the lowest masses ($M \lesssim {\rm
few} \times 10^{6} M_\odot$). TDEs around black holes with the lowest masses
are most likely to reach super-Eddington luminosities at early times in their
evolution. By assuming that the amount of stellar debris which can form into a
compact accretion disc is set dynamically by the Eddington luminosity, we make
a number of interesting and testable predictions about the observed properties
of bright soft-state X-ray TDEs and optically bright, X-ray dim TDEs. We argue
that TDEs around black holes of the lowest masses will expel the vast majority
of their gravitationally bound debris into a radiatively driven outflow. A
large-mass outflow will obscure the innermost X-ray producing regions, leading
to a population of low black hole mass TDEs which are only observed at optical
\& UV energies. TDE discs evolving with bolometric luminosities comparable to
their Eddington luminosity will have near constant (i.e. black hole mass
independent) X-ray luminosities, of order $L_{\rm X, max} \equiv L_M \sim
10^{43} - 10^{44}$ erg/s. The range of luminosity values stems primarily from
the range of allowed black hole spins. A similar X-ray luminosity limit exists
for X-ray TDEs in the hard (Compton scattering dominated) state, and we
therefore predict that the X-ray luminosity of the brightest X-ray TDEs will be
at the scale $L_M(a) \sim 10^{43}-10^{44}$ erg/s, independent of black hole
mass and accretion state. These predictions are in strong agreement with the
properties of the existing population ($\sim 40$ sources) of observed TDEs.
