Final answer:
A protostar becomes a pre-main-sequence star, or T Tauri star, once it has finished accreting mass, before eventually reaching the main-sequence. The stellar evolution of a star like the Sun from main-sequence to red giant and then to white dwarf differs if it is part of a binary system, potentially leading to a supernova.
Step-by-step explanation:
After a protostar has finished accreting mass, it is called a pre-main-sequence star, specifically a T Tauri star for those with masses similar to or less than that of the Sun. T Tauri stars are characterized by being observable mostly in the infrared spectrum due to their dusty envelopes and are in a stage where they are contracting towards the main-sequence. Eventually, the protostar will become a stable main-sequence star like our Sun.
The evolution of a star with mass like that of the Sun from the main-sequence phase includes expansion into a red giant, then shedding its outer layers, and finally ending as a white dwarf. Massive stars follow a slightly different evolutionary path, which can include becoming a type Ia supernova if it is part of a binary system and reaches the Chandrasekhar limit.