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The protoplanetary system HD 169142 is one of the few cases where a potentialcandidate protoplanet has been recently detected via direct imaging. To studythe interaction between the protoplanet and the disk itself observations of thegas and dust surface density structure are needed. This paper reports new ALMAobservations of the dust continuum at 1.3\,mm, $^{12}$CO, $^{13}$CO andC$^{18}$O $J=2-1$ emission from the system HD 169142 at angular resolution of$\sim 0".18 - 0".28$ ($\sim 20\,$au$ - 33\,$au). The dust continuum emissionreveals a double-ring structure with an inner ring between $0".17-0".28$ ($\sim20 - 35\,$au) and an outer ring between $0".48-0".64$ ($\sim 56 - 83\,$au). Thesize and position of the inner ring is in good agreement with previouspolarimetric observations in the near-infrared and is consistent with dusttrapping by a massive planet. No dust emission is detected inside the innerdust cavity ($R \lesssim 20\,$au) or within the dust gap ($\sim 35 - 56\,$au).In contrast, the channel maps of the $J=2-1$ line of the three CO isotopologuesreveal the presence of gas inside the dust cavity and dust gap. The gaseousdisk is also much larger than the compact dust emission extending to $\sim1'.5$ ($\sim 180\,$au) in radius. This difference and the sharp drop of thecontinuum emission at large radii point to radial drift of large dust grains($>$ \micron-size). Using the thermo-chemical disk code \textsc{dali}, thecontinuum and the CO isotopologues emission are modelled to quantitativelymeasure the gas and dust surface densities. The resulting gas surface densityis reduced by a factor of $\sim 30-40$ inward of the dust gap. The gas and dustdistribution hint at the presence of multiple planets shaping the diskstructure via dynamical clearing (dust cavity and gap) and dust trapping(double ring dust distribution).

ALMA unveils rings and gaps in the protoplanetary system HD 169142: signatures of two giant protoplanets