  The star NGC2004#115 in the LMC, originally classified as an (SB1) Be
spectroscopic binary, bears some morphological resemblance to the Galactic
systems LB-1 and HR 6819, both of which are proposed as either Be+black hole
(BH) or Be+stripped He-star systems. Two data-sets (ESO/VLT and SALT) of
multi-epoch optical spectra of NGC 2004#115, separated by baseline of $\sim$20
years, lead us conclude it is a triple system hosting an inner binary with a
period of 2.92 d, eccentricity $\sim$0.0 and mass function $\sim$0.07
$M_\odot$. The inner binary harbours a B-type star (the primary) with projected
rotational velocity of 10km/s, and luminosity $\log L/L_\odot$=3.87,
contributing $\sim$60% of the V-band light to the system. The secondary is not
detected, while the tertiary, which contributes 40% of the light, is
tentatively identified as a less luminous B-type star with high projected
rotational velocity. No ellipsoidal light variability is detected, with
stringent limits being set by MACHO and Gaia data. Assuming the primary to be a
main sequence star yields a mass of 8.6$ M_\odot$, while the additional
assumption of synchronous rotation constrains the inclination to be almost
pole-on with i~9 degrees, implying the secondary is a BH with a mass of
$\sim$25 $M_\odot$. A low mass stripped star with similar luminosity is ruled
out as a potential solution as its mass implies a Roche radius that is
substantially smaller than the stellar radius. The outer period likely exceeds
120 days and, while the disk-like emission is variable (it is almost absent in
the SALT dataset), it may be associated with the inner binary rather than the
rapidly rotating tertiary. XMM-Newton provides an upper limit of 5x$10^{33}$
ergs/s on the X-ray flux, consistent with, though not constraining of, the
system hosting a quiescent B+BH binary. A number of caveats to this scenario
are discussed in the paper.
