  We analyze the properties of 42 rapidly rotating, low metallicity,
quasi-chemically homogeneously evolving stellar models in the mass range
between 4 and 45 $\,\mathrm{M}_\odot$ at the time of core collapse. Such models
were proposed as progenitors for both superluminous supernovae (SLSNe) and long
duration gamma-ray bursts (lGRBs), and the Type Ic-BL supernovae (SNe) that are
associated with them. Our findings suggest that whether these models produce a
magnetar driven SLSN explosion or a near-critically rotating black hole (BH) is
not a monotonic function of the initial mass. Rather, their explodability
varies non-monotonically depending on the late core evolution, once chemical
homogeneity is broken. Using different explodability criteria we find that our
models have a clear preference to produce SLSNe at lower masses, and lGRBs at
higher masses; but find several exceptions, expecting lGRBs to form from stars
as low as 10 $\,\mathrm{M}_\odot$, and SLSNe with progenitors as massive as 30
$\,\mathrm{M}_\odot$. In general, our models reproduce the predicted angular
momenta, ejecta masses and magnetic field strengths at core collapse inferred
for SLSNe and lGRBs, and suggest significant interaction with their
circumstellar medium, particularly for explosions with low ejecta mass.
