  How does molecular complexity emerge and evolve during the process leading to
the formation of a planetary system? Astrochemistry is experiencing a golden
age, marked by significant advancements in the observation and understanding of
the chemical processes occurring in the inner regions of protostellar systems.
However, many questions remain open, such as the origin of the chemical
diversity observed in the early evolutionary stages, which may influence the
chemical composition of the forming planets. Additionally, astrochemistry
provides us with powerful tools to investigate the accretion/ejection processes
occurring in the inner regions of young embedded objects, such as jets, winds,
accretion streamers, and shocks. In this chapter, we review the observational
efforts carried out in recent years to chemically characterize the inner
regions of Solar-System analogs. We summarize our current understanding of
molecular complexity in planet-forming disks and shed light on the existing
limitations and unanswered questions. Finally, we highlight the important role
of future radio facilities, like SKAO and ngVLA, in exploring the chemical
complexity of the regions where planetary systems are emerging.
