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We used a large database extracted from Galaxy-wide surveys of H {\scriptsizeI}, $^{13}$CO 1-0, $8 \micron$ and $870 \micron$ continuum to trace diffuseatomic gas, low- to medium-density molecular gas, high-density molecular gas,and star formation activity which we complemented by dedicated $^{12}$CO 2--1,3--2 observations of the W43 region. From the detailed 3D(space-space-velocity) analysis of the molecular and atomic cloud tracersthrough the region and despite its wide velocity range (\emph{FWHM}$\sim22.3\kms$ around $\vlsr\sim 95.9 \kms$), we identified W43 as a large (equivalentdiameter $\sim 140$ pc) and coherent complex of molecular clouds which issurrounded by an atomic gas envelope (equivalent diameter $\sim 290$ pc). Wemeasured the total mass of this newly-identified molecular complex ($M_{{\tinytotal}}\sim 7.1 \times 10^6 \msun$), the mass contained in dense $870 \micron$clumps ($<5$ pc dense cloud structures, $M_{{\tiny clumps}}\sim 8.4 \times 10^5\msun$) and conclude that W43 is particularly massive and concentrated. Thedistance we assume for the W43 complex is 6 kpc from the Sun, which may placeit at the meeting point of the Scutum-Centaurus (or Scutum-Crux) Galactic armand the Bar, a dynamically complex region where high-velocity streams couldeasily collide. The star formation rate of W43 is suggested not to be steadybut it is increasing from $\, \sim 0.01 \msun\, {yr}^{-1}$ (measured from its$8\,\mu$m luminosity) to $\sim 0.1 \msun\, {yr}^{-1}$ (measured from itsmolecular content). From the global properties of W43, we claim it is anextreme molecular complex in the Milky Way and it could even be formingstarburst clusters in the near future.

W43: the closest molecular complex of the Galactic Bar?