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We reassess the historical $L_{X}/L_{Bol}$ relation for early-type stars froma comparison between T-ReX, the Chandra ACIS X-ray survey of the TarantulaNebula in the LMC, and contemporary spectroscopic analysis of massive starsobtained primarily from VLT/FLAMES, VLT/MUSE and HST/STIS surveys. For 107sources in common (some host to multiple stars), the majority of which arebolometrically luminous (40% exceed $10^6 L_{\odot}$), we find an average $\logL_{X} /L_{Bol} = -6.90 \pm 0.65$. Excluding extreme systems Mk 34 (WN5h+WN5h),R140a (WC4+WN6+) and VFTS 399 (O9 IIIn+?), plus four WR sources withanomalously hard X-ray components (R130, R134, R135, Mk 53) and 10 multiplesources within the spatially crowded core of R136a, $\log L_{X}/L_{Bol} = -7.00\pm 0.49$, in good agreement with Galactic OB stars. No difference is foundbetween single and binary systems, nor between O, Of/WN and WR stars, althoughthere does appear to be a trend towards harder X-ray emission from O dwarfs,through O (super)giants, Of/WN stars and WR stars. The majority of known OBstars in the Tarantula are not detected in the T-ReX point source catalogue, sowe have derived upper limits for all undetected OB stars for which log$L_{Bol}/L_{\odot} \geq 5.0$. A survival analysis using detected andupper-limit log $L_{X}/L_{Bol}$ values indicates no significant differencebetween luminous O stars in the LMC and the Carina Nebula. This analysissuggests that metallicity does not strongly influence $L_{X}/L_{Bol}$. Plasmatemperatures for single, luminous O stars in the Tarantula($\overline{kT_{m}}=1.0$ keV) are higher than counterparts in Carina($\overline{kT_{m}}=0.5$ keV).

X-ray properties of early-type stars in the Tarantula Nebula from T-ReX