  We present a comprehensive review of all observations of the eclipsing
recurrent Nova LMC 1968 in the Large Magellanic Cloud which was previously
observed in eruption in 1968, 1990, 2002, 2010, and most recently in 2016. We
derive a probable recurrence time of $6.2 \pm 1.2$ years and provide the
ephemerides of the eclipse. In the ultraviolet-optical-IR photometry the light
curve shows high variability right from the first observation around two days
after eruption. Therefore no colour changes can be substantiated. Outburst
spectra from 2016 and 1990 are very similar and are dominated by H and He lines
longward of 2000 Angstrom. Interstellar reddening is found to be E(B-V) =
$0.07\pm0.01$. The super soft X-ray luminosity is lower than the Eddington
luminosity and the X-ray spectra suggest the mass of the WD is larger than 1.3
M$_\odot$. Eclipses in the light curve suggest that the system is at high
orbital inclination. On day four after the eruption a recombination wave was
observed in Fe II ultraviolet absorption lines. Narrow line components are seen
after day 6 and explained as being due to reionisation of ejecta from a
previous eruption. The UV spectrum varies with orbital phase, in particular a
component of the He II 1640 Angstrom emission line, which leads us to propose
that early-on the inner WD Roche lobe might be filled with a bound opaque
medium prior to the re-formation of an accretion disk. Both this medium and the
ejecta can cause the delay in the appearance of the soft X-ray source.
