We present astrometry and $BVI$ photometry, down to $Vsimeq22$, of the very young open cluster NGC6530, obtained from observations taken with the Wide Field Imager camera at the MPG/ESO 2.2 m Telescope. Both the $V$ vs. $B-V$ and the $V$ vs. $V-I$ color-magnitude diagrams (CMD) show the upper main sequence dominated by very bright cluster stars, while, due to the high obscuration of the giant molecular cloud surrounding the cluster, the blue envelopes of the diagrams at $Vgtrsim 14$ are limited to the main sequence stars at the distance of NGC6530. This particular structure of the NGC6530 CMD allows us to conclude that its distance is about $d simeq 1250$ pc, significantly lower than the previous determination of d=1800 pc. We have positionally matched our optical catalog with the list of X-ray sources found in a Chandra-ACIS observation, finding a total of 828 common stars, 90% of which are pre-main sequence stars in NGC6530. Using evolutionary tracks of Siess et al. (2000)}, mass and age values are inferred for these stars. The median age of the cluster is about 2.3 Myr; in the mass range (0.6--4.0)$ M_odot$, the Initial Mass Function (IMF) shows a power law index $x=1.22pm0.17$, consistent with both the Salpeter index (1.35), and with the index derived for other young clusters ; towards smaller masses the IMF shows a peak and then it starts to decrease.
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