Embedded clusters are young stellar systems formed within giant molecular clouds (GMCs) and often obscured by dust, making them visible only at infrared wavelengths. Over the past 15 years, advances in infrared astronomy have enabled systematic studies of these clusters. This review summarizes current knowledge about embedded clusters in the Galaxy, including their properties, mass functions, birth rates, and role in star and planet formation. Embedded clusters are defined as groups of stars with a minimum mass density of 1.0 M☉ pc⁻³ and at least 35 members. They are often found in molecular clouds and are typically 0.5–3 Myr old. The catalog of embedded clusters within 2 Kpc of the Sun includes over 100 clusters, with most having masses exceeding 50 M☉ and containing more than 100 members. These clusters account for a significant fraction (70–90%) of all stars formed in GMCs. The mass function of embedded clusters is flat between 50–1000 M☉, suggesting a universal IMF. However, the birth rate of embedded clusters is much higher than that of visible open clusters, indicating a high infant mortality rate. Less than 4–7% of embedded clusters survive to become bound clusters of Pleiades age. The majority of stars in embedded clusters form in rich clusters with masses exceeding 50 M☉. Embedded clusters play a crucial role in studying the initial mass function (IMF), which has been measured over a wide range of stellar and substellar masses. They also provide insights into circumstellar disk evolution and the formation of planetary systems. The internal structure of embedded clusters shows mass segregation, with more massive stars often found near the center. However, the extent of this segregation is not fully understood. The ages and age spreads of embedded clusters are critical for understanding their evolutionary state and star formation history. The age of an embedded cluster provides a lower limit to the age of the molecular cloud from which it formed. Determining the ages of embedded clusters is challenging due to uncertainties in observational data, but they are often estimated using color-magnitude diagrams and theoretical evolutionary tracks. In conclusion, embedded clusters are fundamental to understanding star and planet formation, with significant implications for the IMF, disk evolution, and the formation of bound open clusters. Their study provides valuable insights into the early stages of stellar and planetary system formation.Embedded clusters are young stellar systems formed within giant molecular clouds (GMCs) and often obscured by dust, making them visible only at infrared wavelengths. Over the past 15 years, advances in infrared astronomy have enabled systematic studies of these clusters. This review summarizes current knowledge about embedded clusters in the Galaxy, including their properties, mass functions, birth rates, and role in star and planet formation. Embedded clusters are defined as groups of stars with a minimum mass density of 1.0 M☉ pc⁻³ and at least 35 members. They are often found in molecular clouds and are typically 0.5–3 Myr old. The catalog of embedded clusters within 2 Kpc of the Sun includes over 100 clusters, with most having masses exceeding 50 M☉ and containing more than 100 members. These clusters account for a significant fraction (70–90%) of all stars formed in GMCs. The mass function of embedded clusters is flat between 50–1000 M☉, suggesting a universal IMF. However, the birth rate of embedded clusters is much higher than that of visible open clusters, indicating a high infant mortality rate. Less than 4–7% of embedded clusters survive to become bound clusters of Pleiades age. The majority of stars in embedded clusters form in rich clusters with masses exceeding 50 M☉. Embedded clusters play a crucial role in studying the initial mass function (IMF), which has been measured over a wide range of stellar and substellar masses. They also provide insights into circumstellar disk evolution and the formation of planetary systems. The internal structure of embedded clusters shows mass segregation, with more massive stars often found near the center. However, the extent of this segregation is not fully understood. The ages and age spreads of embedded clusters are critical for understanding their evolutionary state and star formation history. The age of an embedded cluster provides a lower limit to the age of the molecular cloud from which it formed. Determining the ages of embedded clusters is challenging due to uncertainties in observational data, but they are often estimated using color-magnitude diagrams and theoretical evolutionary tracks. In conclusion, embedded clusters are fundamental to understanding star and planet formation, with significant implications for the IMF, disk evolution, and the formation of bound open clusters. Their study provides valuable insights into the early stages of stellar and planetary system formation.