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 2000Å .
Interstellar reddening is found to be E ( B-V ) = 0.07 \pm 0.01 .
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 Å 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 .