The general picture of planet formation is well agreed: planets are formed within a few million years after the collapse phase in a protoplanetary disk surrounding the protostar. However, the detailed formation conditions and mechanisms are still debated, requiring more sophisticated studies both in theoretical, modeling, and observations. A substantial portion of observed exoplanets is found in binary or higher hierarchical systems. Therefore, studying the physical properties and chemical contents of the protoplanetary disk in binary/multiple systems is essential to understand the formation and variety of planetary systems. I will present a study of GG Tauri A using sub-millimeter observations carried out with ALMA and NOEMA interferometers. GG Tauri A is the prototype of a young triple T Tauri star that is surrounded by a massive and extended Keplerian outer disk. The central cavity is not devoid of gas and dust and at least GG Tauri Aa exhibits its own disk of gas and dust emitting at millimeter wavelengths. Its observed properties make this source an ideal laboratory for investigating planet formation in young multiple solar-type stars. A general picture of gas properties and dynamics from the cavity to outer disk as well as its chemical content and the hint of planet(s) in formation in the circumbinary disk of GG Tau A will be presented.